Exploring secular variation of the gravitational constant from high-resolution quasar spectra

The exploration of potential variations in fundamental physical constants is crucial for testing of Grand Unification Theories (GUTs), which aim to unify the fundamental forces of nature. This study utilizes direct observational tests to explore these variations, offering a deep-look into the universe's distant past. By analyzing high-resolution quasar spectra of HE 0515–4414* and comparing them with laboratory-calibrated Ritz wavelengths, we establish an upper limit on the possible cosmological deviation of the gravitational constant: \documentclass[12pt]{minimal} \usepackage{amsmath} \usepackage{wasysym} \usepackage{amsfonts} \usepackage{amssymb} \usepackage{amsbsy} \usepackage{mathrsfs} \usepackage{upgreek} \setlength{\oddsidemargin}{-69pt} \begin{document}$$\dot{\text{G}}/\text{G}=(0.918 \pm 2.830)\times {10}^{-15}{\text{ yr}}^{-1}$$\end{document}G˙/G=(0.918±2.830)×10-15yr-1 over cosmic timescales. Our findings provide a novel tool for probing the physical implications of GUTs, contributing to our understanding of fundamental physics.


Determination of Ġ/G with quasar spectra
The redshifted spectra of quasars offer a valuable tool for investigating spatial and temporal variations in fundamental dimensionless constants, such as the fine-structure constant α and the proton-to-electron mass ratio µ, across cosmic timescales.These constants exhibit sensitivity to change, manifested in resonance states of ions and molecules transitioning to their ground states within these systems.By comparing observed wavelengths with their laboratory values, variations in constants like αcan be directly detected across the universe.Notably, the separation between energy levels, including fine-splitting related to α 4 and the maximum energy level α 2 , is proportionally associated with the redshift.This coupling is fundamentally found in the general relativistic effects of redshift (z) .It can be quantified by the energy (E) loss of a photon, represented as z = −�E/E , where E is the initial energy of the photon.Consequently, this fractional change in energy corresponds to a fractional change in wavelength observations −�E/E = � / ∼ �α/α 39 .Thus, any variations in α can be directly detected across the expanse of the universe by comparing observed wavelengths with their laboratory values [34][35][36][37][38][39] .
Based on the context of Grand Unification Theories (GUTs), we explore the assumption that spatial or temporal variations in fundamental physical constants could provide the potential to unify gravitational and electromagnetic forces.Within this framework, transmutable dimensions are used to determine the weak scale, and all related Yukawa couplings exhibit corresponding variations.We assume that these variations are driven by a dilaton-type mechanism, which in turn impacts the fine-structure constant and the Quantum Chromodynamics (QCD) scale : Here, R can be determined by GUTs.Furthermore, we can derive the value of R through a model-independent approach at low energies, driven by the relationship α(M GUT ) = α s (M GUT ) 34-40 .Moreover, grounded in the concept of dimensional transmutation within the weak scale, we determine that significant variations in Yukawa coupling ( h ) lead to corresponding changes in the Higgs vacuum expectation value ( h).
This, in turn and determines the value of ( ν ) at the Planck scale based on the GUTs of mass.Consequently, we can derive values for where S ≡ dlnν/dlnh, c ≃ ≃ 1 and �h/h = (1/2)�α/α by extension, the electron mass and the proton-to- electron mass ratio variations as As a result, through a perturbative approach, we can obtain variations in the neutron mass m n and the average nucleon mass m N , represented as �m n /m n = �m N /m N = �m p /m p [34][35][36][37][38][39][40] .Collectively, these investigations allow us to infer changes in both α and G over cosmic space-time, their interrelation and the probability of these variations through an in-depth analysis 41 .
In this study, we introduce a set of free phenomenological parameters ( R, S) that are intricately linked to both the Quantum Chromodynamics (QCD) and Electroweak (EW) sectors.These dimensionless coupling exhibit values across various theoretical models and play a crucial role in guiding our analysis.Laboratory determinations of these parameters may exhibit either similar or opposing signs, influencing their application in astrophysical observations.Based on our determined values for R = 273 ± 86 and S = 630 ± 230 , we aim to test the effects of space-time variations in both α and µ with a higher precision.o achieve this, we conduct a comprehensive analysis that couples Ritz wavelengths with observed wavelengths obtained from quasar spectra.We ensure rigorous calibration of wavelengths and quantification of systematic errors during the analytical procedure [42][43][44][45][46] .
We focus our attention on the transition of [Fe II] lines, which are highly suitable candidates for investigating variations in the fundamental constants.These lines are a common observed in quasar spectra and exhibit exceptional sensitivity to variations in essential dimensionless constants, such as the fine-structure constant, the proton-to-electron mass ratio, and the gravitational constant.Their sensitivity often surpasses that of other lines, such as [C I] and [O I] 47 .The advantage of employing [Fe II] lines lies in their consistent line shape, simplifing the definition of parameters used in our analysis and reducing systematic effects.Moreover, the ionization structure or observed substructure of [Fe II] lines is comparatively moderate to other isons, further enhancing their suitability for our anlysis 47 .
Our analytical approach involves combining updated uncertainty error estimations with high-quality [Fe II] spectra 48,49 to achieve a high level of accuracy in estimating systematic errors.We utilize the combined wavelengths of [Fe II] lines derived from quasar spectra and Ritz wavelengths from laboratory measurements.The energy levels relative to [Fe II] are precisely determined through Fourier transform spectroscopy.In our analysis, we indicated that the Doppler shift is used to determine the velocity scale of [Fe II] line spectra derived from quasar observations.In the context of this choice is that the selected [Fe II] lines exhibit uniform velocities, having the same shape, and are characterized by their narrow profiles.To accurately determine their central velocities and linewidths, we employed Gaussian-fitting techniques.Our approach involved the application of a single-fitting Gaussian for single-velocity components and multiple-fitting Gaussians for cases involving multiple-velocity components.Thus, the components of [Fe II] lines were characterized based on their Doppler shift, column density N , absorption redshift z abs , and linewidth b .Progressing step by step, we used the [Fe II] lines to estimate the values �α/α .These values are then intergrated with fitting parameters (R, S, �α/α ) to derive the values of Ġ/G .Our analytical methodology employs a non-linear least-squares fitting approach, combining laboratory measurements with an uncertainty of 10 −6 and observed wavelengths with an uncertainty of 10 −7 .This approach enables precise estimation of the effects of time-variation in the gravitational constant over cosmic timescales.Moreover, we employ a multi-parameter joint analysis approach within a Bayesian framework to comprehensively assess the uncertainties associated with the derived parameters, including �α/α , R, S, and �G/G .This approach allows us to capture the correlations between different parameters and provides a more complete characterization of the parameter space.We begin by defining the parameters of interest and selecting prior distributions based on previous studies and theoretical considerations.These priors guide the analysis and help constrain the parameter space.Using observed data and a likelihood function constructed from observational uncertainties and model assumptions, we derive posterior distributions for each parameter using Bayes' theorem.Markov Chain Monte Carlo (MCMC) sampling techniques are then employed to explore the parameter space and sample from the posterior distributions.The resulting posterior distributions provide insights into the uncertainties of each parameter and quantify the correlations between different parameters, enriching the interpretation of the results in Fig. 1.Finally, we utilize model comparison techniques within the Bayesian framework to assess the goodness-of-fit of different parameter models and select the most suitable model for describing the data [50][51][52][53] .
In our analysis, we focuse on changes in Ġ/G using both minimal ( χ 2 ) and maximal ( χ 2 min ) values with fittingapproximated reductions ( χ 2 ≃ 1 ).We employ �χ 2 = χ 2 − χ 2 min = 1 to evaluate the variation of Ġ/G , deriving maximal variations to simplify the estimation of associated errors.Our study yieldes an upper limit on the time variation of the gravitational constant Ġ/G = (0.918 ± 2.830) × 10 −15 yr −1 , as detailed in Table 1.We estimate both statistical and systematic errors ( σ 2 tot = σ 2 Ġ/G + σ 2 sys ), representing the G variation with redshift in Fig. 2. Figure 2 provides a detailed representation of the effect of time-variation in the gravitational constant Ġ/G , utilizing [Fe II] data lines extracted from observed HE 0515-4414 quasar spectra in combination with Ritz wavelengths.Each data point corresponds to a distinct minimal redshift value.Our analysis methodology is based on independent line ratios associated with and the characteristic line shapes of [Fe II].These line shapes accquire minimal separation, providing a precise estimation of errors, which includes both statistical and systematic errors.The precision of our error estimates is significantly enhanced by evaluating the splitwavelengths for all line pairs of [Fe II].Thus, we can establish the best value of Ġ/G by providing a computational analysis of its sensitivity to time variations concerning χ 2 .In this context, the maximum variation in Ġ/G was calculated by χ 2 − χ 2 min = 1 , incorporating an error estimation approach as follows: �χ 2 = 1 .Subsequently, the smallest value of χ 2 was selected for each fitting procedure, and this value was consistently applied across all fits, with a standard deviation σ 2 tot = σ 2 Ġ/G + σ 2 sys serving as the basis for error estimation in the weighted mean calculation.
In this study, we have presented a potential cosmological variation in the gravitational constant across cosmic timescales.Our analysis has yielded a critical finding Ġ/G = (0.918 ± 2.830) × 10 −15 yr −1 , utilizing the combined wavelengths of [Fe II] and Ritz wavelengths.This result represents the most robust limits on the gravitational constant across various theoretical models, such as Pulsar timing, Lunar Laser Ranging, Big Bang nucleosynthesis, and age of globular clusters [62][63][64][65][66] .Notably, this limit has the potential for even better accuracy compared to current studies through the careful selection of candidates, such as CH 3 OH, OH, and CH molecules [67][68][69][70][71][72][73] .
Future analyses leveraging high-resolution data from astrophysical observations hold the promise of yielding the most reliable estimates of upper bounds on potential spatial and temporal variations of the gravitational constant.Moreover, forthcoming laboratory experiments and enhanced quality of observational data will further constrain variations in dimensionless physical constants.Regardless, this study serves as a valuable tool for testing parameters within unification scenarios [74][75][76] .

Figure 1 .
Figure 1.The plot is for multi-parameter fitting of S R , and �G/G using MCMC sampling.The distributions and covariances of the parameters are shown with 1-sigma (dark blue) and 2-sigma (light blue) confidence intervals.The dashed lines in the histograms represent median values and the 1-sigma confidence range.The true values used for the observational data are R = 273 ± 86 and S = 630 ± 230.

Table 1 .
The determination of Ġ/G was based on the combined Ritz wavlelength of [Fe II] in laboratory and QSO HE 0515-4414 * The result was calculated using the weighted average of all the lines.